标题： 宁静太阳的EUV增亮的空间分布 显示英文标题

标题： Spatial distributions of EUV brightenings in the quiet-Sun

摘要： 太阳轨道器探测到了大量局地瞬态安静太阳日冕中的 EUV 亮事件，这些事件的空间尺度较小，这是太阳轨道器早期的关键研究成果之一。然而，关于这些事件仍然有很多未知之处。 在这里，我们通过研究它们的空间分布，特别是它们是否与光球网络特定的视线磁场拓扑结构共存，来更好地理解 EUV 亮事件。EUV 亮事件使用自动化算法检测，该算法应用于由太阳轨道器极端紫外成像仪于 2022 年 3 月 8 日采集的高时间分辨率（3 秒）数据集，采样时间为约 30 分钟。来自太阳动力学天文台的日震和磁成像仪以及大气成像组件的数据用于提供视线磁场的相关信息和对齐目的。 在这组数据中，我们发现了总共 5064 个 EUV 亮事件，这些事件可以直接与文献中先前报道的事件进行比较。这些事件出现在任何给定帧中的大约 0.015-0.020% 的像素内。我们比较了八个不同的阈值，将 EUV 亮事件分为与视线磁场相关的四个不同类别。使用我们的首选阈值，我们发现有 627 个 EUV 亮事件（占 12.4%）与强双极配置共存，而 967 个 EUV 亮事件（占 19.1%）发生在弱场区域。无论使用什么阈值，只有不到 10% 的 EUV 亮事件与单极视线磁场共存。 在 627 个强双极 EUV 亮事件中，有 54 个事件与消亡共存，而 57 个事件与浮现共存。EUV 亮事件倾向于与光球网络中的强视线磁场共存。然而，它们并不主要与（消亡的）双极共存。 显示英文摘要

摘要： The identification of large numbers of localised transient EUV brightenings, with small spatial scales, in the quiet-Sun corona has been one of the key early results from Solar Orbiter. However, much is still unknown about these events. Here, we aim to better understand EUV brightenings by investigating their spatial distributions, specifically whether they occur co-spatial with specific line-of-sight magnetic field topologies in the photospheric network. EUV brightenings are detected using an automated algorithm applied to a high-cadence (3 s) dataset sampled over ~30 min on 8 March 2022 by the Extreme Ultraviolet Imager's 17.4 nm EUV High Resolution Imager. Data from the Solar Dynamics Observatory's Helioseismic and Magnetic Imager and Atmospheric Imaging Assembly are used to provide context about the line-of-sight magnetic field and for alignment purposes. We found a total of 5064 EUV brightenings within this dataset that are directly comparable to events reported previously in the literature. These events occurred within around 0.015-0.020 % of pixels for any given frame. We compared eight different thresholds to split the EUV brightenings into four different categories related to the line-of-sight magnetic field. Using our preferred threshold, we found that 627 EUV brightenings (12.4 %) occurred co-spatial with Strong Bipolar configurations and 967 EUV brightenings (19.1 %) occurred in Weak Field regions. Fewer than 10 % of EUV brightenings occurred co-spatial with Unipolar line-of-sight magnetic field no matter what threshold was used. Of the 627 Strong Bipolar EUV Brightenings, 54 were found to occur co-spatial with cancellation whilst 57 occurred co-spatial with emergence. EUV brightenings preferentially occur co-spatial with the strong line-of-sight magnetic field in the photospheric network. They do not, though, predominantly occur co-spatial with (cancelling) bi-poles.